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A Study on the Kinematics of Hierarchical Triple Stars
Our statistical analysis shows that, because of the three-body effects,the classical double two-body model cannot be used to describe thekinematics of most hierarchical triple star systems with the precisionof present day observations (1 mas). Even for the usual practicalrequirements, this model is not suitable for figuring those systemssuffering significant three-body effects. Because it is not practical touse numerical ephemerides with a large volume of data to describe thekinematics of component stars in a star catalogue, a kinematical modelas simple and practical as possible for the hierarchical triple starsystems is needed. Based on the existing observations and theirassociated fitting results, we obtain consistent mass parameters andinitial conditions of six hierarchical triple star systems. Then thedescription of the kinematics of these systems on the basis of practicalrequirements is discussed.
| Comparative statistics and origin of triple and quadruple stars
The statistics of catalogued quadruple stars consisting of two binaries(hierarchy 2 + 2), is studied in comparison with triple stars, withrespective sample sizes of 81 and 724. Seven representative quadruplesystems are discussed in greater detail. The main conclusions are asfollows. (i) Quadruple systems of ? Lyr type with similar massesand inner periods are common, in 42 per cent of the sample the outermass ratio is above 0.5 and the inner periods differ by less than 10times. (ii) The distributions of the inner periods in triple andquadruple stars are similar and bimodal. The inner mass ratios do notcorrelate with the inner periods. (iii) The statistics of outer periodsand mass ratios in triples and quadruples are different. The medianouter mass ratio in triples is 0.39 independently of the outer period,which has a smooth distribution. In contrast, the outer periods of 25per cent quadruples concentrate in the narrow range from 10 to 100yr,the outer mass ratios of these tight quadruples are above 0.6 and theirtwo inner periods are similar to each other. (iv) The outer and innermass ratios in triple and quadruple stars are not mutually correlated.In 13 per cent of quadruples both inner mass ratios are above 0.85(double twins). (v) The inner and outer orbital angular momenta andperiods in triple and quadruple systems with inner periods above 30dshow some correlation, the ratio of outer-to-inner periods is mostlycomprised between 5 and 104. In the systems with small periodratios the directions of the orbital spins are correlated, while in thesystems with large ratios they are not. The properties of multiple starsdo not correspond to the products of dynamical decay of small clusters,hence the N-body dynamics is not the dominant process of theirformation. On the other hand, rotationally driven (cascade)fragmentation possibly followed by migration of inner and/or outerorbits to shorter periods is a promising scenario to explain the originof triple and quadruple stars.
| An extremely wide and very low-mass pair with common proper motion. Is it representative of a nearby halo stream?
Aims. We describe the discovery of an extremely wide pair of low-massstars with a common large proper motion and discuss their possiblemembership in a Galactic halo stream crossing the Solar neighbourhood. Methods: In a high proper motion survey of the southern sky we usedmulti-epoch positions and photometry from the SuperCOSMOS Sky Surveys.New nearby ultracool dwarf and subdwarf candidates were selected amongthe faint and red high proper motion objects, and subsequently confirmedby low-resolution classification spectroscopy. The resultingspectroscopic distance estimates, approximate radial velocitymeasurements and improved proper motions involving additional epochsfrom the Two Micron All Sky Survey and from the DEep Near-InfraredSurvey were used to compute Galactic space velocities. Results: Thelate-type (M 7) dwarf SSSPM J2003-4433 and the ultracool subdwarf SSSPMJ1930-4311 (sdM 7) sharing the same very large proper motion of about860 mas/yr were found in the same sky region with an angular separationof about 6°. From the comparison with other high proper motioncatalogues we have estimated the probability of a chance alignment ofthe two new large proper motions to be less than 0.3%. From theindividually estimated spectroscopic distances of about38+10-7 pc and 72+21-16 pc,respectively for the M 7 dwarf and the sdM 7 subdwarf, and in view ofthe accurate agreement in their large proper motions we assume a commondistance of about 50 pc and a projected physical separation of about 5pc. The mean heliocentric space velocity of the pair (U,V,W)=(-232,-170, +74) km s-1, based on the correctness of thepreliminary radial velocity measurement for only one of the componentsand on the assumption of a common distance and velocity vector, istypical of the Galactic halo population. Conclusions: The largeseparation and the different metallicities of dwarfs and subdwarfs makea common formation scenario as a wide binary (later disrupted)improbable, although there remains some uncertainty in the spectroscopicclassification scheme of ultracool dwarfs/subdwarfs so that a dissolvedbinary origin cannot be fully ruled out yet. It seems more likely thatthis wide pair is part of an old halo stream. Higher-resolutionspectroscopic observations are needed to measure accurate radialvelocities of both components. Further, we suggest to check the M 7dwarf for an unresolved binary status, which would explain its shorterspectroscopic distance estimate, and to place both objects on atrigonometric parallax program.Based onobservations with the ESO 3.6 m/EFOSC2 at the European SouthernObservatory, La Silla (ESO program 70.C-0568).
| A methodology for studying physical and dynamical properties of multiple stars. Application to the system of red dwarfs Gl 22
Aims:The main aim of this study is the elaboration of a methodology forstudying physical and dynamical properties of multiple stars and itsapplication to the hierarchical triple system Gl 22. A carefulevaluation of the components' masses and a study of the system's overallstability and long-term dynamical evolution were also pursued. Methods: New NIR speckle interferometric observations with the 6 mtelescope of the Special Astrophysical Observatory (Russia) in the K'photometric band have been carried out. We have made use of the methodfor orbit calculation reported by Docobo (1985). Results: Anoriginal methodology was elaborated and applied to evaluate the mostprobable elements of the outer orbit. Due to the almost definitive orbitof the inner pair, which just covered a full revolution, the motion of Brelative to MCA has been carefully calculated. The positionof MCA was estimated on the basis of differential photometryand empirical mass-luminosity relationships. A weak sinusoidal patternin the apparent motion of the component B was noticed. Conclusions: Our methodology was successfully applied to the triplesystem Gl 22. The newly calculated outer orbit exhibits a moderateeccentricity (e = 0.29), which differs from the previously knowncircular solutions. Both orbits are coplanar and co-revolving. Thisalready known suggestion is now based on a much larger set ofobservational data, including a significant number of specklemeasurements. Gl 22 is most likely a dynamically stable system, at leaston the time scale of 10 Myr. The sinusoidal pattern in the motion of theB component could be caused by a fourth, unseen, very low-mass objectwith a mass of 0.015~M? (16 MJ) on a circularorbit around B with a period of ~15 yr and semimajor axis 0.35 arcsec.
| Speckle Interferometry at the US Naval Observatory. XIII.
The results of 1424 speckle interferometric observations of doublestars, made with the 26 inch (66 cm) refractor of the US NavalObservatory, are presented. Each speckle interferometric observation ofa system represents a combination of over 2000 short-exposure images.These observations are averaged into 1053 mean relative positions andrange in separation from 0.36″ to 61.92″, with a medianseparation of 10.31″. This is the 13th in a series of paperspresenting measurements obtained with this system and covers the period2006 January 12-December 29. Included in these data are nine oldermeasurements whose positions were previously deemed possibly aberrantbut are no longer classified this way following a confirmingobservation. This paper also includes the first data obtained using anew "secondary" camera, designed and built at USNO.
| CCD Measurements of Double and Multiple Stars at NAO Rozhen. III
Using the 2-m telescope of the Bulgarian National AstronomicalObservatory at Rozhen, observations of 55 multiple stars were carriedout during one night, December 16/17. 2006. This is the third series ofCCD measurements of double and multiple stars carried out at Rozhen. Inthe paper we present the results for the position angle and separationfor 49 multiple stars (67 pairs) which could be measured.
| New Distant Companions to Known Nearby Stars. II. Faint Companions of Hipparcos Stars and the Frequency of Wide Binary Systems
We perform a search for faint, common proper motion companions ofHipparcos stars using the recently published Lépine-Shara ProperMotion-North catalog of stars with proper motionμ>0.15'' yr-1. Our survey uncovers a totalof 521 systems with angular separations3''<Δθ<1500'', with 15 triplesand 1 quadruple. Our new list of wide systems with Hipparcos primariesincludes 130 systems identified here for the first time, including 44 inwhich the secondary star has V>15.0. Our census is statisticallycomplete for secondaries with angular separations20''<Δθ<300'' and apparentmagnitudes V<19.0. Overall, we find that at least 9.5% of nearby(d<100 pc) Hipparcos stars have distant stellar companions withprojected orbital separations s>1000 AU. We observe that thedistribution in orbital separations is consistent with Öpik's law,f(s)ds~s-1ds, only up to a separation s~4000 AU, beyond whichit follows a more steeply decreasing power law f(s)ds~s-ldswith l=1.6+/-0.1. We also find that the luminosity function of thesecondaries is significantly different from that of the single stars'field population, showing a relative deficiency in low-luminosity(8
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| Speckle Measurements and Differential Photometry of Visual Binaries with the 6 Meter Telescope of the Special Astrophysical Observatory
Results of speckle measurements and differential photometry carried outwith the 6 m telescope of the Special Astrophysical Observatory (Russia)at the end of 2004 are presented. One new (COU 1569) and four improvedorbits (ADS 440AC, ADS 1729, ADS 5726, and COU 1897), as well as theirdynamical mass estimates, are reported.
| MK Classification and Dynamical Masses for Late-Type Visual Binaries
On the basis of slit spectra obtained with the SCORPIO spectral cameraattached to the 2.6 m telescope of the V. Ambartsumian ByurakanAstrophysical Observatory (Armenia), MK classifications for 30 visualbinaries comprising mostly late K and M type stars are presented.Comparison with other determinations shows that this configurationprovides a reliable MK classification. Dynamical masses for 25 systemsare computed. Using standard mass-luminosity calibrations, individualmass sums for 11 pairs consisting of virtually single, nonvariabledwarfs are calculated, showing a good agreement with correspondingdynamical masses. The dynamical parallax of HIP 112354 is closer to thetrigonometric parallax given in the Yale General Catalogue ofTrigonometric Stellar Parallaxes (van Altena et al.) than to theHipparcos parallax.
| A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)
The LSPM catalog is a comprehensive list of 61,977 stars north of theJ2000 celestial equator that have proper motions larger than 0.15"yr-1 (local-background-stars frame). The catalog has beengenerated primarily as a result of our systematic search for high propermotion stars in the Digitized Sky Surveys using our SUPERBLINK software.At brighter magnitudes, the catalog incorporates stars and data from theTycho-2 Catalogue and also, to a lesser extent, from the All-SkyCompiled Catalogue of 2.5 million stars. The LSPM catalog considerablyexpands over the old Luyten (Luyten Half-Second [LHS] and New LuytenTwo-Tenths [NLTT]) catalogs, superseding them for northern declinations.Positions are given with an accuracy of <~100 mas at the 2000.0epoch, and absolute proper motions are given with an accuracy of ~8 masyr-1. Corrections to the local-background-stars propermotions have been calculated, and absolute proper motions in theextragalactic frame are given. Whenever available, we also give opticalBT and VT magnitudes (from Tycho-2, ASCC-2.5),photographic BJ, RF, and IN magnitudes(from USNO-B1 catalog), and infrared J, H, and Ks magnitudes(from 2MASS). We also provide an estimated V magnitude and V-J color fornearly all catalog entries, useful for initial classification of thestars. The catalog is estimated to be over 99% complete at high Galacticlatitudes (|b|>15deg) and over 90% complete at lowGalactic latitudes (|b|>15deg), down to a magnitudeV=19.0, and has a limiting magnitude V=21.0. All the northern starslisted in the LHS and NLTT catalogs have been reidentified, and theirpositions, proper motions, and magnitudes reevaluated. The catalog alsolists a large number of completely new objects, which promise to expandvery significantly the census of red dwarfs, subdwarfs, and white dwarfsin the vicinity of the Sun.Based on data mining of the Digitized Sky Surveys (DSSs), developed andoperated by the Catalogs and Surveys Branch of the Space TelescopeScience Institute (STScI), Baltimore.Developed with support from the National Science Foundation (NSF), aspart of the NASA/NSF NStars program.
| Multicolour CCD measurements of nearby visual double stars. II
We present accurate CCD astrometric and photometric data for 31 nearbyvisual double stars in the standard filters BVRI. The observations werecollected with a 1.3-m telescope in 2001-2002 The results consist ofrelative astrometric positions (epoch, angular separation and positionangle) and differential BVRI photometry of the components. Mean errorsare: 0.01 arcsec for the separation; 0.06 ° for the position angle;and 0.015m for the photometric data. Comparing the relative positions atdifferent epochs, we evaluate the physical association of the systems.We additionally derive fractional masses and true separations for themost probable binary systems and, whenever orbits are available, alsototal and component masses.Table \ref{t2} is only available in the electronic form athttp:www.edpsciences.org. Tables \ref{t4} and \ref{t5} are onlyavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/422/1023Based on data obtained at the Skinakas Observatory and by the Hipparcosastrometry satellite. The Skinakas Observatory is a collaborativeproject of the University of Crete, the Foundation for Research andTechnology - Hellas, and the Max-Planck-Institut fürExtraterrestrische Physik.
| The Parameterization of the Ground State and Its Applications to Planetary Systems
Natural systems tend to minimize their energy. Hence an importantproblem in astrophysics is the parametrization of the ground state. Inthis context a quantum statistical approach is very useful. The problemof the variational approximation of the density matrix is extendedtowards a parametrization of the ground state. With an analogy to thesemiclassical approach, a classical approach to the variationalprinciple in the parametrization of the ground state is elucidated andits applications are discussed. We find that planetary systems tend tohave circular orbits in an effort to attain the ground state. Theresults of this paper may be useful for the modern problem of detectingplanets around bright stars.
| Empirically Constrained Color-Temperature Relations. I. BV(RI)C
This investigation presents a set of transformations to Johnson B-V,Cousins V-R, and Cousins V-I, as well as bolometric corrections to V,for [Fe/H]=-3, -2, -1, -0.5, 0.0, and +0.3 and, in each case, values oflogg from -0.5 to 5.0 for 3000 K<=Teff<=5500 K and from2.0 to 5.0 for 6000 K<=Teff<=40,000 K. Thesetransformations employ the predictions from Kurucz model atmospheres athigh temperatures (Teff>=8000 K) and from MARCS modelatmospheres at intermediate temperatures (from 7000 K down to atemperature in the range 4000 K<=Teff<=5500 K,depending on [Fe/H], where adjustments to satisfy observationalconstraints become necessary). Thus, theoretical color-Teffrelations are used exclusively down to a minimum temperature that iscooler than the temperatures of turnoff stars in open and globular starclusters. To better represent the color transformations obeyed by coolstars (down to 3000 K), corrections to the synthetic transformationshave been determined from a careful consideration of observations for afew globular clusters (M92, M68, and 47 Tucanae), the color-magnitudediagrams (CMDs) of several open clusters (M67, the Pleiades, the Hyades,and NGC 6791), the CMDs and mass-luminosity diagram for solarneighborhood stars having good distance measurements from Hipparcos,empirical (B-V)-Teff and (V-K)-Teff relations, andcolor-color diagrams for field giants. The semiempirical colortransformations that have been produced as a result of our analysis arealso compared with several others that have been published in recentyears: some of the deficiencies of the latter are revealed.
| Dynamical Masses for Young and Low-mass Stars from Visual Binary Orbits
Not Available
| Visual orbit for the low-mass binary Gliese 22 AC from speckle interferometry
Based on 14 data points obtained with near-infrared speckleinterferometry and covering an almost entire revolution, we present afirst visual orbit for the low-mass binary system Gliese 22 AC. Thequality of the orbit is largely improved with respect to previousastrometric solutions. The dynamical system mass is 0.592+/- 0.065Msun, where the largest part of the error is due to theHipparcos parallax. A comparison of this dynamical mass withmass-luminosity relations on the lower main sequence and theoreticalevolutionary models for low-mass objects shows that both probablyunderestimate the masses of M dwarfs. A mass estimate for the companionGliese 22 C indicates that this object is a very low-mass star with amass close to the hydrogen burning mass limit.Based on observations collected at the German-Spanish AstronomicalCentre on Calar Alto, Spain.
| The association of IRAS sources and 12CO emission in the outer Galaxy
We have revisited the question of the association of CO emission withIRAS sources in the outer Galaxy using data from the FCRAO Outer GalaxySurvey (OGS). The availability of a large-scale high-resolution COsurvey allows us to approach the question of IRAS-CO associations from anew direction - namely we examined all of the IRAS sources within theOGS region for associated molecular material. By investigating theassociation of molecular material with random lines of sight in the OGSregion we were able to construct a quantitative means to judge thelikelihood that any given IRAS-CO association is valid and todisentangle multiple emission components along the line of sight. Thepaper presents a list of all of the IRAS-CO associations in the OGSregion. We show that, within the OGS region, there is a significantincrease ( ~ 22%) in the number of probable star forming regions overprevious targeted CO surveys towards IRAS sources. As a demonstration ofthe utility of the IRAS-CO association table we present the results ofthree brief studies on candidate zone-of-avoidance galaxies with IRAScounterparts, far outer Galaxy CO clouds, and very bright CO clouds withno associated IRAS sources. We find that ~ 25% of such candidate ZOAGsare Galactic objects. We have discovered two new far outer Galaxystar-forming regions, and have discovered six bright molecular cloudsthat we believe are ideal targets for the investigation of the earlieststages of sequential star formation around HII regions. Finally, thispaper provides readers with the necessary data to compare othercatalogued data sets with the OGS data.Tables 1, 2 and A1 are only available in electronic form at the CDS viaanonymous ftp to\ cdsarc.u-strasbg.fr (130.79.128.5) or via\http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/399/1083
| Improved Astrometry and Photometry for the Luyten Catalog. II. Faint Stars and the Revised Catalog
We complete construction of a catalog containing improved astrometry andnew optical/infrared photometry for the vast majority of NLTT starslying in the overlap of regions covered by POSS I and by the secondincremental Two Micron All Sky Survey (2MASS) release, approximately 44%of the sky. The epoch 2000 positions are typically accurate to 130 mas,the proper motions to 5.5 mas yr-1, and the V-J colors to0.25 mag. Relative proper motions of binary components are measured to 3mas yr-1. The false-identification rate is ~1% for11<~V<~18 and substantially less at brighter magnitudes. Theseimprovements permit the construction of a reduced proper-motion diagramthat, for the first time, allows one to classify NLTT stars intomain-sequence (MS) stars, subdwarfs (SDs), and white dwarfs (WDs). We inturn use this diagram to analyze the properties of both our catalog andthe NLTT catalog on which it is based. In sharp contrast to popularbelief, we find that NLTT incompleteness in the plane is almostcompletely concentrated in MS stars, and that SDs and WDs are detectedalmost uniformly over the sky δ>-33deg. Our catalogwill therefore provide a powerful tool to probe these populationsstatistically, as well as to reliably identify individual SDs and WDs.
| Hipparcos red stars in the HpV_T2 and V I_C systems
For Hipparcos M, S, and C spectral type stars, we provide calibratedinstantaneous (epoch) Cousins V - I color indices using newly derivedHpV_T2 photometry. Three new sets of ground-based Cousins V I data havebeen obtained for more than 170 carbon and red M giants. These datasetsin combination with the published sources of V I photometry served toobtain the calibration curves linking Hipparcos/Tycho Hp-V_T2 with theCousins V - I index. In total, 321 carbon stars and 4464 M- and S-typestars have new V - I indices. The standard error of the mean V - I isabout 0.1 mag or better down to Hp~9 although it deteriorates rapidly atfainter magnitudes. These V - I indices can be used to verify thepublished Hipparcos V - I color indices. Thus, we have identified ahandful of new cases where, instead of the real target, a random fieldstar has been observed. A considerable fraction of the DMSA/C and DMSA/Vsolutions for red stars appear not to be warranted. Most likely suchspurious solutions may originate from usage of a heavily biased color inthe astrometric processing.Based on observations from the Hipparcos astrometric satellite operatedby the European Space Agency (ESA 1997).}\fnmsep\thanks{Table 7 is onlyavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/397/997
| The radii and spectra of the nearest stars
We discuss direct measurements of the radii of 36 stars located closerthan 25 parsecs to the Sun. We present the data on 307 radii and 326spectral types and luminosity classes for the nearest stars locatedinside the sphere with a radius of 10 parsecs.
| Revised Coordinates and Proper Motions of the Stars in the Luyten Half-Second Catalog
We present refined coordinates and proper-motion data for the highproper-motion (HPM) stars in the Luyten Half-Second (LHS) catalog. Thepositional uncertainty in the original Luyten catalog is typicallygreater than 10" and is often greater than 30". We have used the digitalscans of the POSS I and POSS II plates to derive more accurate positionsand proper motions of the objects. Out of the 4470 candidates in the LHScatalog, 4323 objects were manually reidentified in the POSS I and POSSII scans. A small fraction of the stars were not found because of thelack of finder charts and digitized POSS II scans. The uncertainties inthe revised positions are typically ~2" but can be as high as ~8" in afew cases, which is a large improvement over the original data.Cross-correlation with the Tycho-2 and Hipparcos catalogs yielded 819candidates (with mR<~12). For these brighter sources, theposition and proper-motion data were replaced with the more accurateTycho-2/Hipparcos data. In total, we have revised proper-motionmeasurements and coordinates for 4040 stars and revised coordinates for4330 stars. The electronic version of the paper5 contains the updated information on all 4470stars in the LHS catalog.
| The Palomar/MSU Nearby Star Spectroscopic Survey. III. Chromospheric Activity, M Dwarf Ages, and the Local Star Formation History
We present high-resolution echelle spectroscopy of 676 nearby M dwarfs.Our measurements include radial velocities, equivalent widths ofimportant chromospheric emission lines, and rotational velocities forrapidly rotating stars. We identify several distinct groups by theirHα properties and investigate variations in chromospheric activityamong early (M0-M2.5) and mid (M3-M6) dwarfs. Using a volume-limitedsample together with a relationship between age and chromosphericactivity, we show that the rate of star formation in the immediate solarneighborhood has been relatively constant over the last 4 Gyr. Inparticular, our results are inconsistent with recent large bursts ofstar formation. We use the correlation between Hα activity and ageas a function of color to set constraints on the properties of L and Tdwarf secondary components in binary systems. We also identify a numberof interesting stars, including rapid rotators, radial velocityvariables, and spectroscopic binaries. Observations were made at the 60inch telescope at Palomar Mountain, which is jointly owned by theCalifornia Institute of Technology and the Carnegie Institution ofWashington.
| Multicolour observations of nearby visual double stars. New CCD measurements and orbits
We present multicolour CCD observations of nine nearby visual doublestars obtained in August and September 1999 with the 1.3-m telescope atSkinakas Observatory. The results consist of relative positions (epochs,angular separations and position angles) and differential BV RIphotometry. We confirm the physical association in eight cases.Previously known orbits do not match the new data for three systems.Orbits have been recalculated when sufficient data were available. Weprincipally improve the precision of the known orbits for three binariesand show the acute lack of precision in two other cases. In one case,the components are shown to move apart with a linear relative speed of0.050\arcsec/yr. Skinakas Observatory is a collaborate project of theUniversity of Crete, the Foundation for Research and Technology -Hellas, and the Max-Planck-Institut für Extraterrestrische Physik.
| Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics
The Catalogue, available at the Centre de Données Stellaires deStrasbourg, consists of 13 573 records concerning the results obtainedfrom different methods for 7778 stars, reported in the literature. Thefollowing data are listed for each star: identifications, apparentmagnitude, spectral type, apparent diameter in arcsec, absolute radiusin solar units, method of determination, reference, remarks. Commentsand statistics obtained from CADARS are given. The Catalogue isavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcar?J/A+A/367/521
| Kinematics of Hipparcos Visual Binaries. I. Stars with Orbital Solutions
A sample consisting of 570 binary systems is compiled from severalsources of visual binary stars with well-known orbital elements.High-precision trigonometric parallaxes (mean relative error about 5%)and proper motions (mean relative error about 3%) are extracted from theHipparcos Catalogue or from the reprocessed Hipparcos data. However, 13%of the sample stars lack radial velocity measurements. Computed galacticvelocity components and other kinematic parameters are used to dividethe sample stars into kinematic age groups. The majority (89%) of thesample stars, with known radial velocities, are the thin disk stars,9.5% binaries have thick disk kinematics and only 1.4% are halo stars.85% of thin disk binaries are young or medium age stars and almost 15%are old thin disk stars. There is an urgent need to increase the numberof the identified halo binary stars with known orbits and substantiallyimprove the situation with their radial velocity data.
| Dynamical Stability of Triple Stars
The dynamical stability of 38 observed hierarchical triple stars withknown orbital elements of the internal and external binary subsystemsand component masses is considered. Four different criteria of dynamicalstability are used. The observed stability parameters and their criticalvalues are calculated by taking into account errors in the orbitalelements and component masses. Most triple systems are stable. Accordingto some criteria, several triple stars (ADS440, xi Tau, lambda Tau,ADS3358, VV Ori, ADS10157, HZ Her, Gliese 795, ADS15971, and ADS16138)may be dynamically unstable. This result is probably associated withunreliability of the empirical stability criteria and/or with errors inthe observed quantities.
| Photometric Measurements of the Fields of More than 700 Nearby Stars
In preparation for optical/IR interferometric searches for substellarcompanions of nearby stars, we undertook to characterize the fields ofall nearby stars visible from the Northern Hemisphere to determinesuitable companions for interferometric phase referencing. Because theKeck Interferometer in particular will be able to phase-reference oncompanions within the isoplanatic patch (30") to about 17th magnitude atK, we took images at V, r, and i that were deep enough to determine iffield stars were present to this magnitude around nearby stars using aspot-coated CCD. We report on 733 fields containing 10,629 measurementsin up to three filters (Gunn i, r and Johnson V) of nearby stars down toabout 13th magnitude at V.
| Catalogue and bibliography of the UV Cet-type flare stars and related objects in the solar vicinity
This new catalogue of flare stars includes 463 objects. It containsastrometric, spectral and photometric data as well as information on theinfrared, radio and X-ray properties and general stellar parameters.From the total reference list of about 3400 articles, partial listsselected by objects, authors, key words and by any pairs of thesecriteria can be obtained Tables 1, 2 and 3 are only available inelectronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html.
| Empirical L-M, R-M, and M-Teff relations for main-sequence stars: Components of close binary systems and low-mass stars
A new catalog of photometric, geometric, and absolute elements of 112detached main-sequence eclipsing variables with known photometric andspectroscopic orbital elements has been combined withspeckle-interferometry data for low-mass stars to yield newmass-luminosity, mass-radius, and mass-spectrum relations: M_bol = 4.46- 9.52 - (lg M > -0.4), M_bol = 6.18 - 5.91 lg M (lg M <= -0.4);lg R = 0.096 + 0.652 lg M (lg M > 0.14), lg R = 0.10 + 1.03 lg M (lgM <= 0.14); lg M = - 5.60 + 1.504 lg T_eff (lg T_eff > 3.6), andlg M = - 29.4 + 8.2 lg T_eff (lg T_eff <= 3.6). In most cases, thecomponent masses and radii used are accurate to 2-3 and 2-4%,respectively; the errors for low-mass stars are larger by factors of3-4. The coefficients in the relations were derived using linear leastsquares fitting with corrections for noise in the independent variable.
| On the possible multiplicity of the components of some low-mass systems
Multiplicity is one factor that can displace a star from the standardmass-luminosity relationship. Assuming that the components of somelow-mass systems whose mass is higher than expected are unresolvedbinaries, we have calculated the most probable values for the masses andluminosities of the hidden components. The calculations are based on atechnique for the minimization of a function of many variables.
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| Csillagkép: | Kassziopeia |
| Rektaszcenzió: | 00h32m29.46s |
| Deklináció: | +67°14'08.1" |
| Vizuális fényesség: | 10.485 |
| Távolság: | 10.128 parszek |
| RA sajátmozgás: | 1741.1 |
| Dec sajátmozgás: | -246.8 |
| B-T magnitude: | 12.158 |
| V-T magnitude: | 10.624 |
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